During threat, interpersonal distance is deliberately increased. Personal space regulation is related to amygdala function and altered in schizophrenia, but it remains unknown whether it is ...particularly associated with paranoid threat.
We compared performance in two tests on personal space between 64 patients with schizophrenia spectrum disorders and 24 matched controls. Patients were stratified in those with paranoid threat, neutral affect or paranoid experience of power. In the stop-distance paradigm, participants indicated the minimum tolerable interpersonal distance. In the fixed-distance paradigm, they indicated the level of comfort at fixed interpersonal distances.
Paranoid threat increased interpersonal distance two-fold in the stop-distance paradigm, and reduced comfort ratings in the fixed-distance paradigm. In contrast, patients experiencing paranoid power had high comfort ratings at any distance. Patients with neutral affect did not differ from controls in the stop-distance paradigm. Differences between groups remained when controlling for gender and positive symptom severity. Among schizophrenia patients, the stop-distance paradigm detected paranoid threat with 93% sensitivity and 83% specificity.
Personal space regulation is not generally altered in schizophrenia. However, state paranoid experience has distinct contributions to personal space regulation. Subjects experiencing current paranoid threat share increased safety-seeking behavior.
The cancellation of noise from terrestrial gravity fluctuations, also known as Newtonian noise (NN), in gravitational-wave detectors is a formidable challenge. Gravity fluctuations result from ...density perturbations associated with environmental fields, e.g., seismic and acoustic fields, which are characterized by complex spatial correlations. Measurements of these fields necessarily provide incomplete information, and the question is how to make optimal use of available information for the design of a noise-cancellation system. In this paper, we present a machine-learning approach to calculate a surrogate model of a Wiener filter. The model is used to calculate optimal configurations of seismometer arrays for a varying number of sensors, which is the missing keystone for the design of NN cancellation systems. The optimization results indicate that efficient noise cancellation can be achieved even for complex seismic fields with relatively few seismometers provided that they are deployed in optimal configurations. In the form presented here, the optimization method can be applied to all current and future gravitational-wave detectors located at the surface and with minor modifications also to future underground detectors.
Terrestrial gravity fluctuations produce so-called Newtonian noise (NN) which is expected to limit the low frequency sensitivity of existing gravitational-waves (GW) detectors LIGO and Virgo, when ...they will reach their full potential, and of next-generation detectors like the Einstein Telescope. In this paper, we present a detailed characterization of the seismic field at Virgo's West End Building as part of the development of a Newtonian noise cancellation system. The cancellation system will use optimally filtered data from a seismometer array to produce an estimate of the Newtonian-noise generated by the seismic field, and to subtract this estimate from the gravitational-wave channel of the detector. By using an array of 38 seismic sensors, we show that, despite the influence of the complexity of Virgo's infrastructure on the correlation across the array, Wiener filtering can still be very efficient in reconstructing the seismic field around the test-mass location. Taking into account the division of the building's foundations into separate concrete slabs, and the different properties of the seismic field across them, we conclude that the arrays to be used for the Newtonian-noise cancellation at Virgo will require a relatively large number of seismometers per test mass, i.e. significantly more than 10. Moreover, observed variations of the absolute noise residuals over time, related to the daily evolution of anthropogenic noise, suggest that the Wiener filter will need to be updated regularly, probably more often than every hour, to achieve stationarity of the background level after subtraction.
In August 2017, Advanced Virgo joined Advanced LIGO for the end of the O2 run, leading to the first gravitational waves detections with the three-detector network. This paper describes the Advanced ...Virgo calibration and the gravitational wave strain h(t) reconstruction during O2. The methods are the same as the ones developed for the initial Virgo detector and have already been described in previous publications, this paper summarizes the differences and emphasis is put on estimating systematic uncertainties. Three versions of the h(t) signal have been computed for the Virgo O2 run, an online version and two post-run reprocessed versions with improved detector calibration and reconstruction algorithm. A photon calibrator has been used to establish the sign of h(t) and to make an independent partial cross-check of the systematic uncertainties. The uncertainties reached for the latest h(t) version are 5.1% in amplitude, 40 mrad in phase and 20 microseconds in timing.
Advanced Virgo is the project to upgrade the Virgo interferometric detector of gravitational waves, with the aim of increasing the number of observable galaxies (and thus the detection rate) by three ...orders of magnitude. The project is now in an advanced construction phase and the assembly and integration will be completed by the end of 2015. Advanced Virgo will be part of a network with the two Advanced LIGO detectors in the US and GEO HF in Germany, with the goal of contributing to the early detections of gravitational waves and to opening a new observation window on the universe. In this paper we describe the main features of the Advanced Virgo detector and outline the status of the construction.
T Accadia et al 2014 Class. Quantum Grav. 31 165013 The Virgo detector is a kilometer-scale interferometer for gravitational wave
detection located near Pisa (Italy). About 13 months of data were ...accumulated
during four science runs (VSR1, VSR2, VSR3 and VSR4) between May 2007 and
September 2011, with increasing sensitivity.
In this paper, the method used to reconstruct, in the range 10 Hz-10 kHz, the
gravitational wave strain time series $h(t)$ from the detector signals is
described. The standard consistency checks of the reconstruction are discussed
and used to estimate the systematic uncertainties of the $h(t)$ signal as a
function of frequency. Finally, an independent setup, the photon calibrator, is
described and used to validate the reconstructed $h(t)$ signal and the
associated uncertainties.
The uncertainties of the $h(t)$ time series are estimated to be 8% in
amplitude. The uncertainty of the phase of $h(t)$ is 50 mrad at 10 Hz with a
frequency dependence following a delay of 8 $\mu$s at high frequency. A bias
lower than $4\,\mathrm{\mu s}$ and depending on the sky direction of the GW is
also present.
The Virgo detector is a kilometer-scale interferometer for gravitational wave detection located near Pisa (Italy). About 13 months of data were accumulated during four science runs (VSR1, VSR2, VSR3 ...and VSR4) between May 2007 and September 2011, with increasing sensitivity. In this paper, the method used to reconstruct, in the range 10 Hz-10 kHz, the gravitational wave strain time series \(h(t)\) from the detector signals is described. The standard consistency checks of the reconstruction are discussed and used to estimate the systematic uncertainties of the \(h(t)\) signal as a function of frequency. Finally, an independent setup, the photon calibrator, is described and used to validate the reconstructed \(h(t)\) signal and the associated uncertainties. The uncertainties of the \(h(t)\) time series are estimated to be 8% in amplitude. The uncertainty of the phase of \(h(t)\) is 50 mrad at 10 Hz with a frequency dependence following a delay of 8 \(\mu\)s at high frequency. A bias lower than \(4\,\mathrm{\mu s}\) and depending on the sky direction of the GW is also present.
grzechów w sakramencie pokuty. Zanika poczucie grzechu, co skutkuje brakiem potrzeby przystępowania do sakramentu pokuty i pojednania. Mimo tych niesprzyjających tendencji europejskiej kultury wiele ...osób wierzących korzysta nadal z tego sakramentu. Z sakramentem pokuty nierozerwalnie związana jest tajemnica spowiedzi nazywana „pieczęcią sakramentalną” (sigillum sacramentale). Artykuł opisuje normy prawne zawarte w Kodeksie Prawa Kanonicznego z 1983 r. oraz Kodeksie Katolickich Kościołów Wschodnich, które w jasny i jednoznaczny sposób określają zakres sigillum i secretum oraz wskazują podmioty zobowiązane do ich zachowania, a także źródła tego zobowiązania. Tajemnica sakramentalna jest nienaruszalna, absolutna do tego stopnia, iż szafarz sakramentu nie tylko nie może zdradzić penitenta i jego grzechów wobec osób trzecich, ale również zabrania się mu korzystania z wiadomości, które pozyskał w związku ze sprawowaniem sakramentu pokuty. Oprócz dyscypliny pokutnej wyznania katolickiego artykuł zawiera próbę ujęcia praktyki pokutnej w Kościołach i wspólnotach eklezjalnych niebędących w jedności ze Stolicą Apostolską. W artykule przedstawiono naukę i przepisy prawne Kościoła prawosławnego i Kościoła Ewangelicko-Augsburskiego na temat pokuty, sposobów jej odprawiania oraz praktyki wyznania grzechów i rozgrzeszenia.
The aim of the present work is to study the influence of a partial substitution of Mn by Zr in MnCoGe alloys. The X-ray diffraction (XRD) studies revealed a coexistence of the orthorhombic ...TiNiSi-type and hexagonal Ni2In- type phases. The Rietveld analysis showed that the changes in lattice constants and content of recognized phases depended on the Zr addition. The occurrence of structural transformation was detected. This transformation was confirmed by analysis of the temperature dependence of exponent n given in the relation ΔSM = C·(BMAX)n. A decrease of the Curie temperature with an increase of the Zr content in the alloy composition was detected. The magnetic entropy changes were 6.93, 13.42, 3.96, and 2.94 J/(kg K) for Mn0.97Zr0.03CoGe, Mn0.95Zr0.05CoGe, Mn0.93Zr0.07CoGe, and Mn0.9Zr0.1CoGe, respectively. A significant rise in the magnetic entropy change for samples doped by Zr (x = 0.05) was caused by structural transformation.
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